EVIDENCE FOR ANCIENT LUNAR BASALTS, P. H. Schultz, Lunarand Planetary Institute, 3303 NASA Road 1, Houston, TX 77058; P. D. Spudis, Department of Geology, Arizona State University, Tempe, AZ 85281 and D. Sellers, Lunar and Planetary Institute, 3303 NASA Road 1 , Houston, TX 77058. Mare basal t units on the Moon are general ly recognized by their 1 ow a1 bedo, a result of the presence of mafic minerals. This fundamental diagnostic obser- vation has been used either implicitly or explicitly to map lunar basal ts and basal tic pyrocl asti cs (1 ) . Where mare basal ts have been buried by crater ejecta deposits, they may be revealed by dark excavated deposits around smaller craters that post date the burial event. The resulting dark-haloed craters have been recognized by numerous 1unar observers (2,3) and are perhaps best i 11 ustrated around Coperni cus , Theophi 1us, and Langrenus (4). The dark-ha1 oed impact craters around Copernicus, in particular, not only reveal the low albedo excavated material but also exhibit the same spectral signature as the local pre-Copernicus basal tic surface. The same approach can be used for larger craters that have excavated more deeply buried deposits. If the crater is too large (D >30 km), then near-surface secondary impact ejecta may dilute the photometric signature of primary crater ejecta. However, near-rim ejecta around smaller craters cannot excavate as large quantities of local material owing to the low impact velocities (v Mare Australe region in the southern 1 unar hemisphere represents a 1arge circular (1 200 km diameter) area containing numerous craters partly inundated by mare basalts. These units exhibit a higher, mottled albedo than most near-side maria and are believed to represent very old units that have lightened with age, at least partly as a result of Humboldt and Jenner crater ejecta (5). Numerous small craters (diameters <15 km) exhibit dark haloes and in a few instances, dark interiors. This contrast between excavated and surface debris suggests that a darker mare basalt unit underlies the exposed higher a1 bedo mare surface. In several examples, dark-haloed craters do not occur on mappable mare units but occur on hummocky lighter plains. Although the dark ejecta deposits might represent a dark mafic unit overlain by 1ighter mare units, the complex geologic history associated with ejecta deposits from enormous craters such as Humboldt suggest that the dark-haloed deposits more 1 i kely correspond to "typical " mare basal ts whose surface has lightened with the accumulation and effects of impact ejecta as originally proposed by Hartman and Wood (6). An inventory of dark-haloed impact craters across both hemispheres of the Moon reveals a wide-spread occurrence. Figure 1 illustrates a region around an unnamed ancient impact basin south of Mare Humorum. At least 14 convincing dark-haloed craters cluster in this general area and typically occur in units mapped as Cay1 ey-type Imbrian Plains material (7). The excavated low-a1 bedo unit clearly pre-dates the Orientale event, as indicated by superposed Oriental e secondary craters. Dark-haloed craters not occurring on mapped mare plains also cluster in other regions of the Moon. The most obvious clusters are north and east of Mare Marginis (Fig. 2), around Mare Crisium, south of Mare Humorum and within Mare Australe, the latter two examples having been, discussed above. Most occur on units previously mapped as Imbrian Plains material .

0 Lunar and Planetary Institute Provided by the NASA Astrophysics Data System ANCIENT BASALTS Schultz, P. H., et al. Orbital Geochemistry Data: The nature of dark crater deposits also can be inferred from the orbital Apollo experiments. Detailed maps of Mg/Si values reveal anomalous local increases west and northeast of Mare Smythii (9) that correlate with cl usters of small dark-haloed craters. Anomalously high concen- trations of Th in terra Cayley-type plains west of Smythii and north of Balmer as seen by the Apollo gamma-ray experiment also correlate with clusters of dark- haloed craters and suggest at least some of these excavated low-albedo deposits may be KREEP-li ke in composition. More impressive is the pronounced mafic anomaly recognized on the farside (115", -8") near Langemak with Mg/Si values approaching typical mare levels with a corresponding decrease in the A1/Si value (10). This geochemical anomaly centers on the crater Vesalius M which exhibits a diffuse, dark ejecta deposit and it is proposed that this crater has excavated mare basalts now buried by old impact debris. Discussion: Virtually all mare basalts returned from the Moon have been dated radiometrically as younger than -3.9 b.y. old, thereby leading many authors to conclude that mare volcanism commenced around this time (1 1) . However, a small percentage of the 1ithic clasts in some Apollo 14 Fra Mauro breccias (-3.95 b.y. old) possess mare basalt chemistry and texture that strongly suggest the existence of pre-Imbrium mare basalt flows perhaps prior to 4.2 b.y. (12). Craters excavating dark materials from below the 1ight highland plains and from below the Orientale ejecta deposits indicate possible examples of such units. Moreover, their widespread occurrence suggests that a large portion of the eastern hemisphere may have been inundated both locally and regionally from southeast of Humboldtianum basin, through Smythii and Balmer basins to Mare Australe. Early topographic studies of 1ight plains units suggested that their origin by non-volcanic processes was supported by the large variations in elevations (13). Figure 3 shows, however, that the distribution of elevations determined from Apoll o-based cartographic data is more uniform for 1i ght plains units than for the maria in the eastern hemisphere. Such uniformity may reflect pre-Imbrium volcanism that has since been masked by the terminal phases of accretion. References : (1 ) Wilhelms D.E. (1970) U. S. Geol. Survey Prof. Paper 599-F, 47 pp. (2) Salisbury J.W., Adler J.E.M. and Smalley V.G. (1968) Royal Astron. Soc. Mon. Nat. 138, 245-249. (3) Head J.W. (1978) Rev. Geophys. Space Phys. 14, 265-300. (4) Schul tz P.H. (1976) Moon ~orphology,U. Texas Press, Austin, 628 pp. (5) Wilhelms D.E. and El Baz F. (1977) U. S. Geol. Survey Misc. Inv. Ser. Map 1-948. (6) Hartmann W.K. and Wood C. (1971) The Moon 3, 3-78. (7) Wilhelms D.E. and McCauley J.F. (1971) U. S. Geol. Survey Misc. Geol. Inv. Map 1-703. (8) Hubbard N. and Conca J. (personal communication). (9) Hubbard N. J., Vilas F. , Keith J. E. (1978) In Mare Crisiwn: The Vim from Luna 24, Pergamon, 13-32. (10) Haines E.L., Etchegaray-Ramirez M. I. and Metzger A.E. (1978) Proc. Lunar Planet. Sci. Conf. 9th, 2985-3013. (11 ) Taylor R. (1975) Lunar Science: A Post-ApoZlo View. Pergamon. 372 pp. (12) Ryder G. and Taylor G. J. (1976) Proc. Lunar Sci. Conf. 7th, 1741-1755. (13) Eqsleton R.E. and Schaber G.G. (1972) In Apollo 16 Prelim. Sci. Rpt., NASA SP-315, 29:7-29:16.

0 Lunar and Planetary Institute Provided by the NASA Astrophysics Data System ANCIENT BASALTS Schul tz, P. H. et a1 .

Fig. la. High-sun earth-based view Fig. 1b. Low-sun Lunar Orbiter showing dark-haloed impact crater (IV-160-HI) view showing 8 km- (top arrow) in smooth plains near diameter crater identified in Schil ler (bottom arrow). Fig. la and rim of Schiller.

0 2 4 6 8 10 12 14 16 18 20 0 2 4 6 8 10 12 14 16 18 20 AREAL PERCENT OF MAPPED UNITS Fig. 2. Location of well-defined Fig. 3. Elevations of mare units dark-ha1 oed impact craters in and light plains units in LAC 43, plains region northeast of Mare 61, 62, 63, and 80 (from LTO data) Marginis. Plains area may represent as a function of relative mapped buried basalt units. area.

0 Lunar and Planetary Institute Provided by the NASA Astrophysics Data System